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Do YSOs host a wide-angled wind? - NIR imaging spectroscopy of H 2 emission -

Subaru UM, 1/30/2008. Do YSOs host a wide-angled wind? - NIR imaging spectroscopy of H 2 emission -. Hiro Takami (ASIAA). 3. Spectro-Imaging using Gemini-NIFS. 1. Introduction. 2. Long-Slit Spectroscopy using Subaru-IRCS. Young stellar objects (HST Public Pictures). Nearby AGN

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Do YSOs host a wide-angled wind? - NIR imaging spectroscopy of H 2 emission -

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  1. Subaru UM, 1/30/2008 Do YSOs host a wide-angled wind?- NIR imaging spectroscopy of H2 emission - Hiro Takami (ASIAA) 3. Spectro-Imaging using Gemini-NIFS 1. Introduction 2. Long-Slit Spectroscopy using Subaru-IRCS

  2. Young stellar objects (HST Public Pictures) Nearby AGN (M87, HST Public Pictures) Distant Galaxy (Subaru Press Release) X-ray binary (SS 433, Courtesy of Amy J. Mioduszewski)

  3. Schematic view of an X-ray binary (Credit: ULTRACAM/VLT ESO) Schematic view of an AGN & jet (http://www.phys.hawaii.edu/~jgl/post/)

  4. 1. Introduction Key Questions (I) • What is the mechanism of mass ejection/accretion? Magneto-centrifugal force (Figs: Shu et al. 1994, Cabrit et al. 1999)

  5. 1. Introduction Key Questions (I) • What is the mechanism of mass ejection/accretion? Magnetic pressure (Uchida & Shibata 1985)

  6. 1. Introduction Key Questions (I) • What is the mechanism of mass ejection/accretion? Magnetic Stress (Hayashi et al. 1996)

  7. 1. Introduction Key Questions (I) • What is the mechanism of mass ejection/accretion? XZ Tau (Goodson et al. 1999) 1” (140 AU) Angular resolutions of present facilities are not sufficient to resolve the central engine. (HST Public Pictures)

  8. 1. Introduction Key Questions (II) • How does the outflow propagate? Are molecular outflows driven by a collimated jet, or an unseen wide-angled wind? Molecular Outflow (Lee et al. 2000) Collimated jet (ESO Archive)

  9. Shocked H2 at the cavity walls? Shocked H2 at the cavity walls? Line Line + Cont. 1. Introduction Observations of a wide-angled wind would be useful to to tackle these issues, but they are not directly observed. UV H2 @ T Tau (Saucedo et al. 2003) H2 2.12 μm @ L1551-IRS5 (Davis et al. 2002)

  10. Instruments • R=1.1x104(dv ~30 km s-1) for Echelle mode, 0”.3 slit Subaru-IRCS • Seeing ~ 0”.7 (AO was not used for our observations) Gemini-NIFS • IFU (FOV=3”x3”), R=5x103(dv ~60 km s-1) • AO-corrected FWHM=0”.1-0”.2

  11. +50 -70 -200 -320 -440 (km s-1) 2. Long-Slit Spectroscopy using Subaru-IRCS • One of the most active T Tauri stars known. H2 emission toward DG Tau (Takami et al. 2004, A&A) (Bacciotti et al. 2000) (Pyo et al. 2003)

  12. 2. Long-Slit Spectroscopy using Subaru-IRCS • One of the most active T Tauri stars known. H2 emission toward DG Tau (Takami et al. 2004, A&A) • Before this study, only 1 star was known as a T Tauri star with NIR H2 emission associated with outflow. • Emission from the other objects are associated with thedisk (or quiescent gas)

  13. 2. Long-Slit Spectroscopy using Subaru-IRCS H2 emission toward DG Tau (Takami et al. 2004, A&A) Spectral Resolution (30 km s-1) (Along the Jet) H2 Continuum (seeing)

  14. 0”.9 0”.6 0”.3 2. Long-Slit Spectroscopy using Subaru-IRCS H2 emission toward DG Tau (Takami et al. 2004, A&A) (Perpendicular to the Jet) H2 Continuum (seeing)

  15. 2. Long-Slit Spectroscopy using Subaru-IRCS • Blueshifted (~15 km s-1) • Measured width (~0”.6) is comparable to the offset (~0”.3) H2 emission toward DG Tau (Takami et al. 2004, A&A) These suggest that warm H2 outflow result from a wide-angled wind. • Shock-excited • UV/X-ray excitation scenarii would not give momentum flux as a T Tauri star

  16. Jet 2 2 Jet 1 1 0 X (arcsec) 0 -1 H2 2.12 um -1 [Fe II] 1.64 um H2 2.12 um -2 -2 -300 -200 -100 0 100 200 300 [Fe II] 1.64 um -300 -200 -100 0 100 200 300 VLSR (km s-1) VLSR (km s-1) 2. Long-Slit Spectroscopy using Subaru-IRCS • Observed kinematic structures are similar to T Tauri stars (but those at HH sources show lower excitation) H2 & [Fe II] emission @ HH sources(Takami et al. 2006, ApJ)

  17. 600 600 300 300 X (AU) X (AU) 0 0 -300 -300 -300 -300 -300 -300 -300 -300 -200 -200 -200 -200 -200 -100 -200 -100 -100 0 -100 -100 0 100 -100 0 100 200 0 100 0 200 0 100 200 100 200 100 200 200 300 300 300 300 300 300 VLSR (km s-1) VLSR (km s-1) VLSR (km s-1) VLSR (km s-1) VLSR (km s-1) VLSR (km s-1) 2. Long-Slit Spectroscopy using Subaru-IRCS • Acceleration over hundreds AU suggest that this is an entrained component by an unseen wide-angled wind (or jet). H2 & [Fe II] emission @ HH sources(Takami et al. 2006, ApJ)

  18. H2(color) jet Continuum (blue contour) 3. Integral-Field Spectroscopy using Gemini-NIFS H2 emission toward six T Tauri stars (Beck, McGregor, Takami, Pyo 2008, ApJ)

  19. 3. Integral-Field Spectroscopy using Gemini-NIFS H2 emission toward six T Tauri stars (Beck, McGregor, Takami, Pyo 2008, ApJ) • A variety of morphology • associated with jets, winds and ambient gas • Excitation temperature ~2000 K → shock excited

  20. E N (x10) (x10) 1” 1” (x5) H2 (x10) 3. Integral-Field Spectroscopy using Gemini-NIFS Detailed Study for HL Tau (Takami et al. 2007, ApJL) [Fe II] H2 (original) (unsharp-masked) Continuum (1.64 m)

  21. [Fe II] H2 1” Spectral resolution -200 -100 0 100 VHel (km s-1) H2(gray) [Fe II] (contour) H2(gray) Cont. 1.64μm(contour)

  22. 3. Integral-Field Spectroscopy using Gemini-NIFS Detailed Study for HL Tau (Takami et al. 2007, ApJL) • Presence of “micro molecular bipolar H2 flow” is revealed • H2 emission in some regions are associated with the cavity walls. • There is no evidence for kinematic interaction with the collimated jet. A wide-angled wind interacts with ambient material, opening up cavities.

  23. SiO J=2-1 (white) SO NJ=56-45(red) NIR H2(blue) CO J=1-0 (white) CO J=2-1 (green) (Lee et al. 2006) (Dutrey et al. 1997) Conclusion and Future Directions • NIR H2 emission toward some active YSO results from an unseen wide-angled wind • Extensive studies would be useful to discuss best strategy for ALMA studies

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